Zeitschriftenartikel: „Astronomical spectroscopy“

1

Bhattacharyya, J. C. „Astronomical spectroscopy“. Resonance 3, Nr. 6 (Juni 1998): 16–24. http://dx.doi.org/10.1007/bf02836981.

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2

Bhattacharyya, J. C. „Astronomical spectroscopy“. Resonance 3, Nr. 5 (Mai 1998): 24–29. http://dx.doi.org/10.1007/bf02838839.

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3

Miller, David J. „Astronomical spectroscopy: an introduction to the atomic and molecular physics of astronomical spectroscopy“. Contemporary Physics 61, Nr. 4 (01.10.2020): 304. http://dx.doi.org/10.1080/00107514.2020.1853241.

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4

Panchuk, V. E., M. E. Sachkov, M. V. Yushkin und M. V. Yakopov. „Integral methods in astronomical spectroscopy“. Astrophysical Bulletin 65, Nr. 1 (Januar 2010): 75–94. http://dx.doi.org/10.1134/s1990341310010074.

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5

Allamandola, L. J. „Grain Spectroscopy“. Symposium - International Astronomical Union 150 (1992): 65–72. http://dx.doi.org/10.1017/s0074180900089725.

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Our fundamental knowledge of interstellar grain composition has grown substantially during the past two decades thanks to significant advances in two areas: astronomical infrared spectroscopy and laboratory astrophysics. The opening of the mid-infrared, the spectral range from 4000-400 cm−1 (2.5-25 μm), to spectroscopic study has been critical to this progress because spectroscopy in this region reveals more about a material's molecular composition and structure than any other physical property.

6

Odeh, Mohammad Sh. „Low cost equipment for astronomical spectroscopy“. Journal of Instrumentation 16, Nr. 12 (01.12.2021): T12009. http://dx.doi.org/10.1088/1748-0221/16/12/t12009.

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Abstract The purpose of this paper is to show how we can obtain spectra for different astronomical objects using low coat equipment. Where a high-efficiency diffraction grating named “The Star Analyzer” was used by the International Astronomical Center (IAC) in Abu Dhabi, UAE to get the spectrum of different astronomical objects. Balmer series was readily visible when observing an “A” type star. TiO absorptions lines were distinguished by observing an “M” type star. Methane absorption lines were visible by observing Uranus and Neptune. Whereas HI and HeI emission lines were detected by observing a blue hypergiant. In addition, C2 Swan band absorption lines were identified by observing a red giant carbon star. This type of observation is very interesting for public outreach as well as university students, because it shows astrophysical principles for public and students practically and by using low cost equipment.

7

Hentschel, Klaus. „Updating a handbook on astronomical spectroscopy“. Journal for the History of Astronomy 46, Nr. 2 (Mai 2015): 242–43. http://dx.doi.org/10.1177/0021828614552243.

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8

Glaspey, John W., und Ian Powell. „A camera for astronomical CCD spectroscopy“. Publications of the Astronomical Society of the Pacific 100 (Oktober 1988): 1282. http://dx.doi.org/10.1086/132317.

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9

DEVORKIN, D. „Astronomical Spectroscopy: The Analysis of Starlight.“ Science 237, Nr. 4816 (14.08.1987): 783–84. http://dx.doi.org/10.1126/science.237.4816.783-a.

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10

Martin-Drumel, M. A., K. L. K. Lee, A. Belloche, O. Zingsheim, S. Thorwirth, H. S. P. Müller, F. Lewen et al. „Submillimeter spectroscopy and astronomical searches of vinyl mercaptan, C2H3SH“. Astronomy & Astrophysics 623 (März 2019): A167. http://dx.doi.org/10.1051/0004-6361/201935032.

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Context. New laboratory investigations of the rotational spectrum of postulated astronomical species are essential to support the assignment and analysis of current astronomical surveys. In particular, considerable interest surrounds sulfur analogs of oxygen-containing interstellar molecules and their isomers. Aims. To enable reliable interstellar searches of vinyl mercaptan, the sulfur-containing analog to the astronomical species vinyl alcohol, we investigated its pure rotational spectrum at millimeter wavelengths. Methods. We extended the pure rotational investigation of the two isomers syn and anti vinyl mercaptan to the millimeter domain using a frequency-multiplication spectrometer. The species were produced by a radiofrequency discharge in 1,2-ethanedithiol. Additional transitions were remeasured in the centimeter band using Fourier-transform microwave spectroscopy to better determine rest frequencies of transitions with low-J and low-Ka values. Experimental investigations were supported by quantum chemical calculations on the energetics of both the [C2,H4,S] and [C2,H4,O] isomeric families. Interstellar searches for both syn and anti vinyl mercaptan as well as vinyl alcohol were performed in the EMoCA spectral line survey carried out toward Sgr B2(N2) with ALMA. Results. Highly accurate experimental frequencies (to better than 100 kHz accuracy) for both syn and anti isomers of vinyl mercaptan are measured up to 250 GHz; these deviate considerably from predictions based on extrapolation of previous microwave measurements. Reliable frequency predictions of the astronomically most interesting millimeter-wave lines for these two species can now be derived from the best-fit spectroscopic constants. From the energetic investigations, the four lowest singlet isomers of the [C2,H4,S] family are calculated to be nearly isoenergetic, which makes this family a fairly unique test bed for assessing possible reaction pathways. Upper limits for the column density of syn and anti vinyl mercaptan are derived toward the extremely molecule-rich star-forming region Sgr B2(N2) enabling comparison with selected complex organic molecules.

11

Polińska, M., K. Kamiński, W. Dimitrov, M. Fagas, W. Borczyk, T. Kwiatkowski, R. Baranowski, P. Bartczak und A. Schwarzenberg–Czerny. „Global Astrophysical Telescope System – GATS“. Proceedings of the International Astronomical Union 9, S301 (August 2013): 475–76. http://dx.doi.org/10.1017/s1743921313015123.

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AbstractThe Global Astronomical Telescope System is a project managed by the Astronomical Observatory Institute of Adam Mickiewicz University in Poznań (Poland) and it is primarily intended for stellar medium/high resolution spectroscopy. The system will be operating as a global network of robotic telescopes. The GATS consists of two telescopes: PST 1 in Poland (near Poznań) and PST 2 in the USA (Arizona). The GATS project is also intended to cooperate with the BRITE satellites and supplement their photometry with spectroscopic observations.

12

Sharda, Prashast, Tanisha Tyagi und Naresh Kumari. „Medical and Astronomical Applications of Raman Spectroscopy“. International Journal of Advanced Engineering Research and Applications 5, Nr. 02 (30.06.2019): 50–55. http://dx.doi.org/10.46593/ijaera.2019.v05i02.001.

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The main purpose of this paper is to study the applications of Raman Spectroscopy in the fields of medicine and astronomy. These applications show the involvement of Raman Spectroscopy, rendering qualitative and quantitative aspects of various fields like medicine, astronomy, geosciences, defense etc. These applications have proven to be lucrative in the said fields; such as, by determining the health of an unborn child in the medical field. It has helped many astronomers in uncovering the various secrets of the cosmos as well. The ability of Raman spectroscopy to probe the vibration modes of emission of different molecules either by absorption or emission spectra has innumerable applications which will be discussed further in the paper, in order to give the readers a complete panorama of the field with respect to its applications.

13

Stepkin, S. V. „Digital Sign Correlator for Radio Astronomical Spectroscopy“. Telecommunications and Radio Engineering 52, Nr. 5 (1998): 47–51. http://dx.doi.org/10.1615/telecomradeng.v52.i5.60.

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14

Gully-Santiago, Michael A., Jessica L. Luna, Caroline V. Morley, Kyle Kaplan, Aishwarya Ganesh, Erica A. Sawczynec, Joel Burke und Daniel M. Krolikowski. „Astronomical échelle spectroscopy data analysis with muler“. Journal of Open Source Software 7, Nr. 73 (12.05.2022): 4302. http://dx.doi.org/10.21105/joss.04302.

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15

Cabezas, C., C. Bermúdez, Y. Endo, B. Tercero und J. Cernicharo. „Rotational spectroscopy and astronomical search for glutaronitrile“. Astronomy & Astrophysics 636 (April 2020): A33. http://dx.doi.org/10.1051/0004-6361/202037769.

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Context. Nitriles constitute almost 15% of the molecules observed in the interstellar medium (ISM), surprisingly only two dinitriles have been detected in the ISM so far. The lack of astronomical detections for dinitriles may be partly explained by the absence of laboratory rotational spectroscopic data. Aims. Our goal is to investigate the rotational spectrum of glutaronitrile, N≡C−CH2−CH2−CH2−C≡N, in order to allow its possible detection in the ISM. Methods. The rotational spectrum of glutaronitrile was measured using two different experimental setups. A Fourier transform microwave spectrometer was employed to observe the supersonic jet rotational spectrum of glutaronitrile between 6 and 20 GHz. In addition, the mmW spectrum was observed in the frequency range 72−116.5 GHz using a broadband millimetre-wave spectrometer based on radio astronomy receivers with fast Fourier transform backends. The spectral searches were supported by high-level ab initio calculations. Results. A total of 111 rotational transitions with maximum values of J and Ka quantum numbers 54 and 18, respectively, were measured for the gg conformer of glutaronitrile. The analysis allowed us to accurately determine the rotational, nuclear quadrupole coupling, quartic and sextic centrifugal distortion constants. These rotational parameters were employed to search for glutaronitrile in the cold and warm molecular clouds Orion KL, Sgr B2(N), B1-b and TMC-1, using the spectral surveys captured by IRAM 30 m at 3 mm. Glutaronitrile was not detected, and the upper limits’ column densities were derived. Those are a factor of 1.5 and 5 lower than those obtained for the total column densities of the analogous succinonitrile in Orion KL and Sgr B2, respectively.

16

Lee, David, Roger Haynes, Deqing Ren und Jeremy Allington‐Smith. „Characterization of Lenslet Arrays for Astronomical Spectroscopy“. Publications of the Astronomical Society of the Pacific 113, Nr. 789 (November 2001): 1406–19. http://dx.doi.org/10.1086/323908.

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17

Vrtilek, J. M., P. Thaddeus und C. A. Gottlieb. „Laboratory and Astronomical Spectroscopy of Reactive Hydrocarbons“. Symposium - International Astronomical Union 120 (1987): 87–88. http://dx.doi.org/10.1017/s0074180900153835.

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The rotational spectra of C3H2, C3H, and C2D, molecules not previously studied, were investigated in a continuing program of mm-wave spectroscopy in space and in the laboratory of hydrocarbons of astrophysical interest. Laboratory measurements producing reactive species in a DC glow discharge through organic gases have been essential to the identification of these species.

18

Pounds, K. A. „Astronomical X-ray spectroscopy—ten years on“. Vistas in Astronomy 33 (Januar 1990): 83–103. http://dx.doi.org/10.1016/0083-6656(90)90039-b.

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19

HOLT, STEPHEN S. „New Frontiers in X-Ray Astronomical Spectroscopy“. Annals of the New York Academy of Sciences 655, Nr. 1 Frontiers in (Juni 1992): 263–77. http://dx.doi.org/10.1111/j.1749-6632.1992.tb17076.x.

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20

Maillard, J. P. „Recent results in astronomical Fourier transform spectroscopy“. Spectrochimica Acta Part A: Molecular and Biomolecular Spectroscopy 51, Nr. 7 (Juli 1995): 1105–15. http://dx.doi.org/10.1016/0584-8539(94)00014-3.

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21

Naylor, David A., Brad G. Gom, Matthijs H. D. van der Wiel und Gibion Makiwa. „Astronomical imaging Fourier spectroscopy at far-infrared wavelengths“. Canadian Journal of Physics 91, Nr. 11 (November 2013): 870–78. http://dx.doi.org/10.1139/cjp-2012-0571.

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The principles and practice of astronomical imaging Fourier transform spectroscopy (FTS) at far-infrared wavelengths are described. The Mach–Zehnder (MZ) interferometer design has been widely adopted for current and future imaging FTS instruments; we compare this design with two other common interferometer formats. Examples of three instruments based on the MZ design are presented. The techniques for retrieving astrophysical parameters from the measured spectra are discussed using calibration data obtained with the Herschel–SPIRE instrument. The paper concludes with an example of imaging spectroscopy obtained with the SPIRE FTS instrument.

22

Murphy, Michael T., Clayton R. Locke, Philip S. Light, Andre N. Luiten und Jon S. Lawrence. „Laser frequency comb techniques for precise astronomical spectroscopy“. Monthly Notices of the Royal Astronomical Society 422, Nr. 1 (12.03.2012): 761–71. http://dx.doi.org/10.1111/j.1365-2966.2012.20656.x.

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23

Clampin, M., und R. P. Edwin. „Large format imaging photon detector for astronomical spectroscopy“. Review of Scientific Instruments 58, Nr. 2 (Februar 1987): 167–73. http://dx.doi.org/10.1063/1.1139302.

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24

Roesler, F. L., R. J. Reynolds und F. Scherb. „Fabry-Perot Spectroscopy of Extremely Faint Astronomical Sources“. International Astronomical Union Colloquium 149 (1995): 95–106. http://dx.doi.org/10.1017/s0252921100022739.

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AbstractOur interests in the general field of astrophysics lie principally in two areas: 1) the study of extremely faint emission lines from the interstellar medium, galactic halo, and intergalactic clouds, and 2) the study of neutral and ionized components of the outer atmospheres of solar system objects, including the earth. These studies require instruments of the highest possible area-solid angle product, but typically do not require extremely high spatial resolution. This paper highlights our past work in these areas, and discusses new instrumental approaches we are developing.

25

Bernath, Peter F. „Molecular opacities for exoplanets“. Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 372, Nr. 2014 (28.04.2014): 20130087. http://dx.doi.org/10.1098/rsta.2013.0087.

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Spectroscopic observations of exoplanets are now possible by transit methods and direct emission. Spectroscopic requirements for exoplanets are reviewed based on existing measurements and model predictions for hot Jupiters and super-Earths. Molecular opacities needed to simulate astronomical observations can be obtained from laboratory measurements, ab initio calculations or a combination of the two approaches. This discussion article focuses mainly on laboratory measurements of hot molecules as needed for exoplanet spectroscopy.

26

Huenemoerder, David. „Archiving CCD/Electronic Astronomical Data“. Highlights of Astronomy 9 (1992): 713–14. http://dx.doi.org/10.1017/s1539299600010133.

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The availability and advances in two-dimensional electronic detectors, in particular the charge-coupled-devices (CCDs), are a great asset to astronomical imaging and spectroscopy because of their sensitivity, dynamic range, and linearity. In some cases photographic plates still offer an advantage to imaging of large size, but the advent of large format CCDs may make a figure of merit, the area per exposure time, much more favorable for CCDs.

27

Gatkine, Pradip, Sylvain Veilleux und Mario Dagenais. „Astrophotonic Spectrographs“. Applied Sciences 9, Nr. 2 (15.01.2019): 290. http://dx.doi.org/10.3390/app9020290.

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Astrophotonics is the application of photonic technologies to channel, manipulate, and disperse light from one or more telescopes to achieve scientific objectives in astronomy in an efficient and cost-effective way. Utilizing photonic advantage for astronomical spectroscopy is a promising approach to miniaturizing the next generation of spectrometers for large telescopes. It can be primarily attained by leveraging the two-dimensional nature of photonic structures on a chip or a set of fibers, thus reducing the size of spectroscopic instrumentation to a few centimeters and the weight to a few hundred grams. A wide variety of astrophotonic spectrometers is currently being developed, including arrayed waveguide gratings (AWGs), photonic echelle gratings (PEGs), and Fourier-transform spectrometer (FTS). These astrophotonic devices are flexible, cheaper to mass produce, easier to control, and much less susceptible to vibrations and flexure than conventional astronomical spectrographs. The applications of these spectrographs range from astronomy to biomedical analysis. This paper provides a brief review of this new class of astronomical spectrographs.

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Ludwig, Hans-Günter. „Book Review: "Astronomical Spectroscopy — An Introduction to the Atomic and Molecular Physics of Astronomical Spectra"“. Journal of Astronomical Instrumentation 04, Nr. 03n04 (Dezember 2015): 1580001. http://dx.doi.org/10.1142/s225117171580001x.

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29

Watson, William D. „Astronomical spectroscopy: Interstellar space contains the largest encountered atoms“. Nature 315, Nr. 6021 (Juni 1985): 630–31. http://dx.doi.org/10.1038/315630b0.

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30

Prato, M., M. Piana, A. G. Emslie, G. J. Hurford, E. P. Kontar und A. M. Massone. „A Regularized Visibility-Based Approach to Astronomical Imaging Spectroscopy“. SIAM Journal on Imaging Sciences 2, Nr. 3 (Januar 2009): 910–30. http://dx.doi.org/10.1137/090746355.

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31

Cosby, P. C., und T. G. Slanger. „OH spectroscopy and chemistry investigated with astronomical sky spectra“. Canadian Journal of Physics 85, Nr. 2 (01.02.2007): 77–99. http://dx.doi.org/10.1139/p06-088.

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This study summarizes the use of a large catalog of astronomical sky spectra to study different aspects of OH spectroscopy and chemistry in the terrestrial night sky. The sky spectra are unique in that they have high spectral resolution, cover the entire visible wavelength region in one exposure, and are intensity-calibrated with respect to standard stars. The intensity calibration, in particular, allows a significant revision to the OH Meinel band intensity distribution that has been in use for 43~years and permits critical evaluation of the many available sets of OH emission coefficients. The spectra further allow the OH rovibrational population distributions to be monitored throughout many nights. The OH vibrational population distribution is found to change during the night, with the population ratio between the extreme high-v and low-v levels that we can detect, v = 9 and v = 3, varying by as much as a factor of two; the low-v levels being predominant earlier in the night. It has been common to determine the kinetic temperature of the OH emission region by assuming that it is equal to the low-J rotational temperature associated with particular OH bands, typically bands originating in the v = 6 and v = 8 levels. The present calibrated data set reveals that the rotational temperatures are significantly greater for high-v than for low-v levels, the typical difference between v = 3 and v = 8 being 15 K. Previous attempts to establish that a difference existed are consistent with our current observations, although conclusions from those earlier results were limited by relatively wide error limits. The present rovibrational population measurements, which extend to high rotational levels (J′ ≤ 25.5), also reveal that the high-J populations are largely independent of vibrational level — the high-J population in v = 3 is similar to that in v = 7.PACS Nos.: 92.60.H, 92.60.hw, 33.20.–t, 33.20.Kf, 33.70.–w

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Kagi, Eriko, Yasuko Kasai, Hans Ungerechts und Kentarou Kawaguchi. „Astronomical Search and Laboratory Spectroscopy of the FeCO Radical“. Astrophysical Journal 488, Nr. 2 (20.10.1997): 776–80. http://dx.doi.org/10.1086/304735.

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33

Chechelnitsky, A. M. „Horizons and new possibilities for astronomical system's mega spectroscopy“. Advances in Space Research 29, Nr. 12 (Juni 2002): 1917–22. http://dx.doi.org/10.1016/s0273-1177(02)00247-8.

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34

Melosso, Mattia, Brett A. McGuire, Filippo Tamassia, Claudio Degli Esposti und Luca Dore. „Astronomical Search of Vinyl Alcohol Assisted by Submillimeter Spectroscopy“. ACS Earth and Space Chemistry 3, Nr. 7 (03.06.2019): 1189–95. http://dx.doi.org/10.1021/acsearthspacechem.9b00055.

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35

Maillard, J. P. „Signal-to-Noise Ratio and Astronomical Fourier Transform Spectroscopy“. Symposium - International Astronomical Union 132 (1988): 71–78. http://dx.doi.org/10.1017/s0074180900034793.

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The multiplex properties of the Fourier Transform Spectrometer (FTS) can be considered as disadvantageous with modern detectors and large telescopes, the dominant noise source being no longer in most applications the detector noise. Nevertheless, a FTS offers a gain in information and other instrumental features remain: flexibility in choosing resolving power up to very high values, large throughput, essential in high–resolution spectroscopy with large telescopes, metrologic accuracy, automatic substraction of parasitic background. The signal–to–noise ratio in spectra can also be improved: by limiting the bandwidth with cold filters or even cold dispersers, by matching the instrument to low background foreoptics and high–image quality telescopes. The association with array detectors provides the solution for the FTS to regain its full multiplex advantage.

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Puzzarini, Cristina. „Astronomical complex organic molecules: Quantum chemistry meets rotational spectroscopy“. International Journal of Quantum Chemistry 117, Nr. 2 (12.09.2016): 129–38. http://dx.doi.org/10.1002/qua.25284.

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37

Politsch, Collin A., Jessi Cisewski-Kehe, Rupert A. C. Croft und Larry Wasserman. „Trend filtering – I. A modern statistical tool for time-domain astronomy and astronomical spectroscopy“. Monthly Notices of the Royal Astronomical Society 492, Nr. 3 (14.01.2020): 4005–18. http://dx.doi.org/10.1093/mnras/staa106.

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ABSTRACT The problem of denoising a 1D signal possessing varying degrees of smoothness is ubiquitous in time-domain astronomy and astronomical spectroscopy. For example, in the time domain, an astronomical object may exhibit a smoothly varying intensity that is occasionally interrupted by abrupt dips or spikes. Likewise, in the spectroscopic setting, a noiseless spectrum typically contains intervals of relative smoothness mixed with localized higher frequency components such as emission peaks and absorption lines. In this work, we present trend filtering, a modern non-parametric statistical tool that yields significant improvements in this broad problem space of denoising spatially heterogeneous signals. When the underlying signal is spatially heterogeneous, trend filtering is superior to any statistical estimator that is a linear combination of the observed data – including kernel smoothers, LOESS, smoothing splines, Gaussian process regression, and many other popular methods. Furthermore, the trend filtering estimate can be computed with practical and scalable efficiency via a specialized convex optimization algorithm, e.g. handling sample sizes of n ≳ 107 within a few minutes. In a companion paper, we explicitly demonstrate the broad utility of trend filtering to observational astronomy by carrying out a diverse set of spectroscopic and time-domain analyses.

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Bernath, Peter F. „SpS1-Laboratory spectroscopy of small molecules“. Proceedings of the International Astronomical Union 5, H15 (November 2009): 541–42. http://dx.doi.org/10.1017/s1743921310010628.

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This contribution focuses on the study of ‘cool’ sources with surface temperatures in the range of about 500-4000 K. In this temperature range spectra are dominated by strong molecular absorption and the tools of modern chemical physics can be applied to compute the molecular opacities needed to simulate the observed spectral energy distributions. (See Bernath (2005) for an introduction to molecular spectroscopy including line intensities and Bernath (2009) for a recent astronomical review article.)

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McGuire, Brett A., Marie-Aline Martin-Drumel, Sven Thorwirth, Sandra Brünken, Valerio Lattanzi, Justin L. Neill, Silvia Spezzano et al. „Molecular polymorphism: microwave spectra, equilibrium structures, and an astronomical investigation of the HNCS isomeric family“. Physical Chemistry Chemical Physics 18, Nr. 32 (2016): 22693–705. http://dx.doi.org/10.1039/c6cp03871a.

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40

Qibin, Li. „New Initiatives in Astronomical Facilities in China“. Highlights of Astronomy 11, Nr. 2 (1998): 890–91. http://dx.doi.org/10.1017/s1539299600019031.

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Proposals on future astronomy facilities have been surveyed in China recent years. Among the others, the Large Multi-Object Spectroscopy Telescope (LAMOST) has been cosidered to have higher priority by the astronomical community because of its optimum fit of large aperture and large field of view (POV) in the design. The LAMOST has been approved as a national project this year.

41

Schönfelder, V. „Gamma-Ray Line Spectroscopy Results from COMPTEL“. Symposium - International Astronomical Union 188 (1998): 35–38. http://dx.doi.org/10.1017/s0074180900114378.

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Comptel aboard NASA's Compton Observatory has led to a major progress in the field of astronomical gamma-ray line spectroscopy. Highlights are the all-sky map of the 1.8 MeV line from radioactive 26Al, the first detection of the 1.156 MeV line from radioactive 44Ti from a Supernova remnant (Cas A), and the detection of excessive MeV emission from the Orion complex that may be ascribed to excitation of 12C and 16O nuclei.

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Cvetojevic, Nick, Nemanja Jovanovic, Jon Lawrence, Michael Withford und Joss Bland-Hawthorn. „Developing arrayed waveguide grating spectrographs for multi-object astronomical spectroscopy“. Optics Express 20, Nr. 3 (17.01.2012): 2062. http://dx.doi.org/10.1364/oe.20.002062.

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43

Tulloch, S. M., und V. S. Dhillon. „On the use of electron-multiplying CCDs for astronomical spectroscopy“. Monthly Notices of the Royal Astronomical Society 411, Nr. 1 (03.11.2010): 211–25. http://dx.doi.org/10.1111/j.1365-2966.2010.17675.x.

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44

Sarre, Peter J. „The diffuse interstellar bands: A major problem in astronomical spectroscopy“. Journal of Molecular Spectroscopy 238, Nr. 1 (Juli 2006): 1–10. http://dx.doi.org/10.1016/j.jms.2006.03.009.

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45

Wells, Tyler, und Paul L. Raston. „Concerning the asymmetric top rotational partition function in astronomical spectroscopy“. Journal of Molecular Spectroscopy 370 (April 2020): 111292. http://dx.doi.org/10.1016/j.jms.2020.111292.

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46

Monnet, G. „3D Spectroscopy with large Telescopes: past, present and prospects“. International Astronomical Union Colloquium 149 (1995): 12–17. http://dx.doi.org/10.1017/s0252921100022600.

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AbstractThe dimensional curse of having to pack 3D spectrophotometry data on solely 2D detectors is briefly discussed, and the main astronomical domains covered by 3D spectroscopy introduced. Finally, the scientific case for high spatial resolution 3D techniques coupled to Adaptive Optics capabilities is presented, with special emphasis on the observation of the nuclei of galaxies.

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Viotti, Roberto. „Archiving and Distribution of Spectroscopic Data“. Highlights of Astronomy 9 (1992): 727–28. http://dx.doi.org/10.1017/s1539299600010194.

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Spectroscopy is a fundamental tool for the investigation of physical conditions in astronomical objects. Up to the present a considerable amount of information has been collected, which could be of great help in research in all fields of Astrophysics. There is however the problem of safeguarding such material, to create ad hoc archives of raw and/or reduced spectral data, and to have homogenised means of documentation and of distribution of the material to the Astronomical Community. These problems were discussed by members of the IAU Commission 29, Stellar Spectra, during the 21st IAU General Assembly, and the results are herewith summarized.

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Bebekovska, Elena Vchkova, Galin Borisov, Zahary Donchev und Gordana Apostolovska. „Preliminary Results of Low Dispersion Asteroid Spectroscopy Survey at NAO Rozhen“. Proceedings of the International Astronomical Union 12, S330 (April 2017): 395–96. http://dx.doi.org/10.1017/s174392131700566x.

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AbstractWe are presenting the first results of low dispersion spectroscopic observation of asteroids at Bulgarian National Astronomical Observatory Rozhen. Asteroids with unclassified spectra and brighter than 15 magnitude have been chosen. Besides just presenting the asteroid reflectance, classification according to Bus S. J. et al. (2012) has been done. The asteroid spectra of 590 Tomyris, 703 Noemi, 1596 Itzigsohn and 1826 Miller are presented together with standard spectra corresponding to the three best matches given by the public software tool M4AST (Popescu M. et al. (2012)). Our aim is to participate in the coordinated program of asteroids spectroscopy complementary to the observations of Gaia.

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Dubosq, C., C. Falvo, F. Calvo, M. Rapacioli, P. Parneix, T. Pino und A. Simon. „Mapping the structural diversity of C60 carbon clusters and their infrared spectra“. Astronomy & Astrophysics 625 (Mai 2019): L11. http://dx.doi.org/10.1051/0004-6361/201834943.

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The current debate about the nature of the carbonaceous material carrying the infrared (IR) emission spectra of planetary and proto-planetary nebulae, including the broad plateaus, calls for further studies on the interplay between structure and spectroscopy of carbon-based compounds of astrophysical interest. The recent observation of C60 buckminsterfullerene in space suggests that carbon clusters of similar size may also be relevant. In the present work, broad statistical samples of C60 isomers were computationally determined without any bias using a reactive force field, their IR spectra being subsequently obtained following local optimization with the density-functional-based tight-binding theory. Structural analysis reveals four main structural families identified as cages, planar polycyclic aromatics, pretzels, and branched. Comparison with available astronomical spectra indicates that only the cage family could contribute to the plateau observed in the 6–9 μm region. The present framework shows great promise to explore and relate structural and spectroscopic features in more diverse and possibly hydrogenated carbonaceous compounds, in relation with astronomical observations.

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Terwisscha van Scheltinga, J., N. F. W. Ligterink, A. C. A. Boogert, E. F. van Dishoeck und H. Linnartz. „Infrared spectra of complex organic molecules in astronomically relevant ice matrices“. Astronomy & Astrophysics 611 (März 2018): A35. http://dx.doi.org/10.1051/0004-6361/201731998.

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Context. The number of identified complex organic molecules (COMs) in inter- and circumstellar gas-phase environments is steadily increasing. Recent laboratory studies show that many such species form on icy dust grains. At present only smaller molecular species have been directly identified in space in the solid state. Accurate spectroscopic laboratory data of frozen COMs, embedded in ice matrices containing ingredients related to their formation scheme, are still largely lacking.Aim. This work provides infrared reference spectra of acetaldehyde (CH3CHO), ethanol (CH3CH2OH), and dimethyl ether (CH3OCH3) recorded in a variety of ice environments and for astronomically relevant temperatures, as needed to guide or interpret astronomical observations, specifically for upcoming James Webb Space Telescope observations.Methods. Fourier transform transmission spectroscopy (500–4000 cm−1/20–2.5 μm, 1.0 cm−1 resolution) was used to investigate solid acetaldehyde, ethanol and dimethyl ether, pure or mixed with water, CO, methanol, or CO:methanol. These species were deposited on a cryogenically cooled infrared transmissive window at 15 K. A heating ramp was applied, during which IR spectra were recorded until all ice constituents were thermally desorbed.Results. We present a large number of reference spectra that can be compared with astronomical data. Accurate band positions and band widths are provided for the studied ice mixtures and temperatures. Special efforts have been put into those bands of each molecule that are best suited for identification. For acetaldehyde the 7.427 and 5.803 μm bands are recommended, for ethanol the 11.36 and 7.240 μm bands are good candidates, and for dimethyl ether bands at 9.141 and 8.011 μm can be used. All spectra are publicly available in the Leiden Database for Ice.

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